Occuttau'on@NewsteuerVolume III, Number 9 November, 1984

Occultation Newsletter is published by the International Occultation Timing Association. Editor and compos-itor: H. F. DaBo11; 6 N 106 White Oak Lane; St. Charles, IL 60174; U. S. A. Please send editorial matters,renewals, address changes, and reimbursement requests to the above, but for new memberships, new subscrip-tions, back issues, and any special requests, write to IOTA; P. 0. Box 3392; Columbus, OH 43210-0392; U.S.A.

FROM THE PUBLISHER

For subscription purposes, this is the third issueof 1984.

When renewing, please give your name and address ex-actly as it appears on your mailing label, so thatwe can locate your file; if the label should be re-vised, tell us how it should be changed.

o.n.'s price is $1.40/issue, or $5.50/year (4 is-sues) including first class surface mailing. Backissues through vol. 2, No. 13 still are priced atonly $1.00/issue; later issues @ $1.40. Please seethe masthead for the ordering address. Air mailshipment of o.n. back issues and subscriptions, ifdesired, is 45¢/issue ($1.80/year) extra, outsidethe U.S.A., Canada, and Mexico.

IOTA mwbership, subscription included, is $11.00/year for residents of North America (including Mexi-co) and $16.00/year for others, to cover costs ofoverseas air mail. Observers from Europe and theBritish Isles should join IOTA/ES, sending DM 20.--to Hans-j. Bode, Bartold-knaust Str. 8, 3000 Hanno-ver 91, German Federal Republic.

IOTA NEWS

David Id. Dunham~

This year's meeting of the International OccultationTiming Association will be held at the Lunar andPlanetary Institute in Houston, TX, on Saturday, Oc-tober 20th, starting at 10 am. More details weregiven on p. 157 of the last issue. Unfortunately,my schedule has prevented me from sending my materi-al to the editor early enough for this issue toreach most subscribers before the meeting.

Planning for the three IOTA expeditions to observethe total solar eclipse on November 22-23rd is near-ly complete, and if you have not already joined oneof the expeditions, it my be too late by the timeyou receive this. Paul Maley is leading an expedi-tion of about two dozen observers from North Ameri-ca; they plan to observe just inside the northernlimit near Port Moresby. David Herald and ByronSoulsby are leading an Australian expedition, de-parting from Sydney on November 21 for six days.Arrangements have been made to observe near thesouthern limit in Papua New Guinea. Hans Bode's Eu-ropean expedition will cost 5970 DM (a little under$2000), including all expenses for 12 days, some ofwhich will be in Bali (a shorter duration may be

possible). The round-trip air fare from Amsterdam toDjakarta is about 1500 DM, included in the totalprice. They hope to observe near the southern limitin West Irian. Alan Fiala and I expect to computeand distribute detailed predictions of the path,taking the lunar profile into account, in October.He also hope to reduce a small amount of data fromthe May 30th eclipse to estimate an empirical cor-rection to the prediction. We now have a prelimi-nary master record of the central two or three min-utes of several video records of the May 30theclipse, which has been (or soon will be) distribut-ed to those who sent us videotapes; others who wanta copy can obtain one by sending one of us a blankvideotape cassette, preferably VHS format. See page165 of the last issue. lde may have a more completeversion ready in time for the IOTA meeting, and willdistribute it back to those who sent us tapes, un-less they need the preliminary version sooner for apresentation. We apologize for the delay in produc-ing this, and the expanded profile plots which willbe needed in order to analyze the data.

I understand that IOTA/ES has applied to become atax-exwpt scientific organization in the FederalRepublic of Germany, as IOTA has done in the U.S.A.Forms for validating tax-deductible travel expensesto make scientifically useful observations of occu1-tations and eclipses will be distributed to IOTAmembers in the U.S.A. (and to anyone else who re-quests them) with the next issue, targeted for lateNovember or early December (it will include predic-tion lists for 1985 planetary and asteroidal occu1-tations). At least a preliminary version of theform will be available at the IOTA meeting.

Peter Manly. 1533 W. 7th Street, Tempe, AZ 85281,telephone 602,966-3920, has prepared a package ofinformation, including circuit diagrams and bro-chures from some companies, describing equipment andconnectors to be used with video cameras or VCR'S.The equipment inserts time to the nearest 0.01 sec-ond, and a bar which varies in length according tothe amplitude of the audio signal. The bar jumps atclear time signal seconds beats, and therefore canbe used to calibrate the time display. The packageweighs 8 ounces, and Peter will send a copy to any-one who sends him the necessary postage ($1.39 forfirst class in North America). Sending a large (9by 12 inches) self-addressed manila envelope willhelp. Paul Maley notes that JVC now has a simple0.01-second timer for use with JVC equipment forabout $100, and it apparently can be used with RCAUltricon cameras with one or two simple connections.An article by Manly about astronomically useful vid-

180

co equipment will appear in the November issue ofAstronomy magazine, and the December issue will con-tain another article presenting some video observa-tional results, including occultations.

Again, the article on graze expedition results hashad to be postponed; some graze information has beenincluded (see pp. 188 and 190). I apologize for thedelay. Even more neglected have been reports ofprogress with double stars relating to occultations.But David S. Evans has published a definitive arti-cle on double stars discovered with photoelectricobservations of lunar occultations in Lowell Qbser·vatory Bulletin No. 167, "Current Techniques in Dou-ble and Multiple Star Research" edited by R. Har-rington and 0. Franz, p. 63. This bulletin is actu-ally the 296-page proceedings of the I.A.U. Collo-quium No. 62 held at Lowell in 1981. Evans' arti-cle, "The Discovery of Double Stars at Occulta-tions," includes a 16-page catalog of all photoelec-tric observations of stars, for which at least oneof the observers has claimed possible duplicity, ob-tained from the literature. Negative observationsof the same star are included. The catalog is ar-ranged in order of SAD number. Another useful re-cent publication is "Fourth Catalog of Orbits ofVisual Binary Stars," by C. Worley and Id. Heintz,Publications of usno Second Series Vol. XXIV — PartVII (1983). I do plan to publish an article aboutnew doubles discovered during occultations, not inthe next issue but, I hope, in o.n. 3 (ii), early in1985.

MAY was off the air on all frequencies on August20th from 5:25 to 6:02 UT and on August 22-23rd from23:49 to 0:08 UT, according to the National Bureauof Standards' Time and Frequency Bulletin No. 322(Sept. 1984). So if you had trouble timing some oc-cultations then, now you know why. KMVH had no out-ages during August. I recomnend wearing a digitalwatch with an alarm. If you can't receive time sig-nals and are using a tape recorder, set the alarm togo off a minute or two before the predicted event,and record the alarm. With the tape recorder stillrecording, set the alarm again to go off at thefirst available minute after the observing period,and record it. [Ed: Alternatively, you could leavethe watch in minute-alarm-set mode, pushing the re-set button shortly after the alarm sounds the min-ute, leaving it ready to announce the next one.This would limit the tape recorder drift to thatwhich could occur in a single minute.] Then cali-brate the watch a few times (such as by recordingthe alarm and accurate time signals) as soon as pos-sible after the event, doing this for a period oftime longer than the time from the event to thefirst calibration. North Americans can telephone900,4)0-TIME if they can't receive any of the short-wave time signals.

The experience with the occultation by (47) Aglajademonstrated the need to remain flexible (see page182). Near the times of observationally promisingevents, even ones nominally predicted to occur farfrom your location, avoid scheduling important ac-tivities. Budget the time for less-urgent work,which could be postponed if astrometric updates showthat the path will be over, or within trave11ingdistance of your location. Try to keep informedabout updates (remind the coordinator for your re-gion that you want to be informed. Even if no as-trometric observations have been' made, plan to moni-

tor the star around the predicted time of closestapproach, weather permitting. Isolated observationsof secondary occultations continue to be reported;these will be confirmed only by greater efforts bymore observers, including attempts at separatedpairs of stations. Plan to spend much more timethan you think necessary to find the star; practiceduring previous nights, and a good finder (prefera-bly at least 8 x SO), facilitate this. Frequentlycheck the weather (both the latest forecast and thelatest observations), no matter how pessimistic itseems; fronts often move faster or slower than pre-dicted.

Offices are being changed again at Computer SciencesCorporation, where I work. My daytime telephonentmber is now 301,589-1545, ext. 392 (no longer603). If you can't reach me at my extension, youcan have me paged or leave a message that youcalled. Or you can call my home telephone, 301,585-0989, where a recording machine will take your mes-sage if nobody can answer it.

ANYONE FOR VISA OR MASTERCARD?

Brian Loader, Blenheim, New Zealand, has suggestedthat we could have an arrangwent to charge IOTAdues or o.n. subscription and back issue paymentsvia VISA or MasterCard. This might be of advantage,especially to foreign residents, as it might avoidsome rather substantial bank charges for foreign ex-change, and probably would avoid much of the hassleof getting a bank draft. However, such charge serv-ice is not free. IOTA would have to pay 4% to thebank for each such charge. U. S. lawmakers tend tolegislate against increasing prices only for cardusers, but do not object to giving discounts tothose not using the cards. It would be necessaryfor us to raise all rates by 4%, but anyone not us-ing the charge could take a 3.846% discount from thenew rates, bringing the effective rates back to thecurrent rates. Individuals could authorize thecharge by letter, but should not expect us to returna standard receipt, which would not show anythingbut the U. S. funds amount, anyway; the local cur-rency amount would have to be determined from themonthly statement. Each individual would have todetermine whether or not the charge arrangementwould be advantageous to him.

This is an item for discussion at the IOTA annualbusiness meeting, and for approval or disapproval bythe Board of Directors of IOTA. The result will beannounced in o.n., either in the next issue, or asa last-minute addition to this one. (See p. 190.)

ANALYSIS AND PUBLICATION OFOBSERVATIONS REPORTED TO IOTA

David Id. Dunham

When occultation or eclipse observations are report-ed to me, or to others who are designated to collectthe observations for IOTA (such as jim Stam in thecase of asteroidal appulse observations, see page185), it is assumed that I am, or someone workingwith me is, free to analyze and publish the observa-tions, unless the observer states some restrictionswhen he su*its his report. Usually, only approxi-mate information and preliminary results are pub-lished first in o.n. Final analyses of importantevents observed from several locations, such as to-

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and asteroidal occultations, usually will be submitted for publication in refereed pro-fessional journals. My general guideline for the author list of such articles is to in-clude all who participated in the analysis, those who accurately recorded the observa-tions with automatic equipment (such as photometers and video cameras), regional coordi-nators who reported useful visual observations made by others as well as by themselves,and professional astronomers who make especially significant visual observations. Allobservers, visual or automatic, whose data are included in the article will be creditedby name in the article. I believe this policy is fair; let me know if you have anyquestions about it.

UPCOMING PLANETARY OCCULTATIONS

David W. Dunham

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Information about three occultations during December is given here in tables like thoseused and described in o.n. 3 (6), 120 and following. Some data about the occultationsby (4) Vesta and (717) Wisibada were given on pages 158 and 159 of the last issue, butthe December 30th date of the Vesta occultation was omitted. The errors in Landgraf's

occultation calculations described on p. 160 of the last issue turned

f- - out to be due to the fact that he used ephemeris data at ten-day inter-° """ vals, which is all right for the calculation of asteroid orbits, but is= L) CVmW

uu8 2u·)_ tOO coarse for occultation calculations. When he generated his ephem-

m " ' eris data at one-day intervals, his occultation calculations were in< ajnjc·j good agreement with mine. Some notes about particular events, some ofQ.a E,d&r: which were listed in o.n. 3 (6), are given below.

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< ""2 Oct. 6, (365) Corduba- According to an improved orbit for this aster-e e° old calculated by. Id. Landgraf, this occultation did not occur, the

= "S path missing the earth's surface by over 3". A finder chart was givencc ' on p. 176 of the last issue, but no regional map for the U.S.A. wasCJ·kj LA · - ·

4- ,\J generated, since we knew that the EMP 1982 orbit was inaccurate. If5e b the path from Landgraf's data had been more favorable, we would have'n'n + tried to distribute a shorter version of this issue earlier, or other-& · "r wise to have notified potential observers before the event.&& SX8!2 :- Nov. 19, Venus: The regional map published on p. 178 of the last issue

S2 # did not extend far enough east, so a revised version is published in

U,j 5== this issue, See also p. 160 of the last issue.

. = Dec. I, (717) Wisibada: Normally, we would not bother with an asteroid" & "E this small. However, otherwise observing circumstances and the path

< a kS for this occultation are very favorable, so observations are encour-+¥ aged. If astrometry half as good as that for the September 16th occu1-

p- 2 2 tation by (47) Aglaja (see pb. 182) is obtained for Wisibada, the nar-m row path could be predicted accurately enough to target mobile observ-cD Le)

v, <c ~ ers. The good accuracy of the 18-inch Lowell astrograph may force us" to reconsider the lower limit of asteroid sizes used in occultationO

= &1 gs2g search programs. Wisibada could serve as a good test case. Inform-" """ tion about the occultation, including a finder chart, will be published~b m 8&Y in the November issue of Sky and Telescope. The stellar diameter pa-x EI t"" rameters are 0.17 milli-arc seconds, 205 meters, 22 milliseconds, and

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f- j- &o=, Dec. 16, (184) Dejopeja: The diameter of Dejopeja could be anywhereu, ~ com,o from 36 km to 132 km, depending on whether it is in the E, M, or P~~ S "= class. Observations of this occultation, potentially visible from Eu-

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cl. e aoa Dec. 29, (747) wi'nchestier: This occultation was identified during-? ,o,ou, late scans at Lowell Observatory; see p. 162 of the last issue. Since

w 'i' "&= Ehe AGK3 field covering this event is shown in the middle of p. 176 of,=, S m the last issue, only the A.C. field identifying the star is published

" i'n this Tssue.Z ¢U4.jm V)

~ Q) m Q)E S :2=Ag PROPOSED CHANGES FOR ASTEROIDAL OCCULTATION PREDICTIONS FOR 19852: ell C c,n

·m·r Q)""" David Id. Dunham^~Kr

~ X:Z Several observers have complained about the length of the prediction" :se "= lists, making it hard to decide which events theij should attempt to ob-:a c7\<C g) cj g, serve. Many of the events involve faint stars with small magnitudeE "" 22& drops in bright moonlight. Those in North America and Europe should

182

concentrate mainly on events for which finder chartsare published. The list of events for which astrom-etry is planned, such as on p. 160 of the last is-sue, can also serve as a guide.

For 1985, I plan to be more selective in the eventsI list, considering angular diameter and duration aswell as the observational circumstances noted above.In addition, events which likely can be detected on-ly photoelectrically will be included neither ino.n. nor in the local circumstance predictions dis-tributed by Joseph Carroll, but instead will be dis-tributed separately to the smaller number of observ-ers who can use them. The "visual" events will berestricted to Am's greater than 0.4 for 7th-magni-tude stars, 0.6 for 9th-mag., 0.8 for 11th mag., and1.0 for 13th mag.; no stars fainter than 13.0 willbe included, although occultations of them might beseen with very large telescopes, most of which areoutfitted with photometers, anyway. These Am re-strictions will not be applied for occultations byplanets which have a significant dark side (defectof illumination exceeding 1!'0). Predictions for oc-cultations with smaller Am's will be published in aseparate Supplement for photoelectric observers. Itwill be sent free to IOTA members whom I know tohave a photoelectric capability, or who request itfrom the editor-treasurer (see address in masthead).Occultation Newsletter subscribers who are not IOTAmembers will have to pay $1.00 per year to subscribeto the photoelectric Supplement, and overseas sub-scribers in this category will need to pay an addi-tional amount to cover airmail postage. Except forspecial objects, occultations with Nn less than0.05, or involving stars fainter than magnitude14.0, will not be included in the Supplement. Also,the Atlas-Coeli parts of the finder charts will notbe included for these events, since virtually allphotoelectric observers have access to these or moredetailed charts, and usually don't need them sincethey normally work with well-calibrated setting cir-cles.

If you have any connents or objections to the pro-posed chanjjes, write to me at P.0. Box 7488, SilverSpring, MD 20907, U.S.A. There will be no changesuntil November, when I will produce the 1985 predic-tions for the next o.n.

I plan to give the positions of the stars to moreaccuracy, to the nearest second of time in R.A. andto O:i in dec., to help identify faint stars incrowded fields. This will be done only for the 1950positions., unless someone can give me a good reasonfor also giving the apparent positions to greateraccuracy.

I plan to create a large catalog including all AGK3and SAD stars, as well as many from other catalogs.I plan to use it for producing the finder chartswhich are now generated with either SAD or AGK3 da-ta. This should eliminate the problem of missingbright stars from my AGK3 data (some stars in theprinted AGK3 are not in the magnetic tape versionobtained from the Astronomisches Rechen Institut,and vice versa) and the 10° declination zone bound-aries of my SAD data. These problems now are takencare of manually for the charts published in o.n.,but observers outside of North America and Europeoften rely on the raw computer-produced charts whichI distribute.

THE SEPTEMBER 16TH OCCULTATIONOF SAD 146599 BY (47) AGLAJA

David Id. Dunham

Regional maps and a finder chart for this occulta-tion were published on pages 170 and 171 of the lastissue. Astrometric observations were made at LowellObservatory during the nights before the occultationusing the newly mounted 18-inch telescope describedon pages 161 and 162 of the last issue. The pathpredicted by Bob Mi11is and Ted Bowell from theireleven exposures had a shift value of 1!'05 south andtime correction of 2.8 minutes early, placing thepath across the southern U.S.A., England, northernGermany, and southern Denmark. Larry Wasserman'spreliminary solution from a few of the observationsof the occultation show that the prediction from theastrometric observations was in error by only 0!'004,probably the best-predicted asteroidal occultationto date!

When Millis telephoned me on the 13th with the firstprediction, we coordinated efforts to notify as manypotential observers as possible. Since the long-range weather forecast was pessimistic in the U.S.A.east of Texas, efforts were concentrated more in thewestern part of the path. With help from WolfgangBeisker, we got word to European coordinators. Un-fortunately, it was cloudy in Germany, Holland, andBelgium. Some miss observations reported from Den-mark might constrain the northern limit, whose loca-tion is known only poorly from the American data.

Several astronomers left Lowell Observatory on the14th, heading for southeastern New Mexico to deploytheir three portable photoelectric systems. I madereservations to fly to Texas for the event, but can-celled these plans when I learned that the weatherforecast, as of 12 hours before the occultation, wasthat a cold front would be along or just south ofthe path from Arizona to the Carolinas, with no goodclearing until a few hours after the event. Thisalso discouraged my notificqtion effort. But sixhours before the occultation, checking with theweather office indicated that the front was movingfaster than expected, with mostly clear skies ex-pected from northern Georgia to Mississippi and westof central Texas. With help from my wife, Joan, Iwas able to pack observing equipment and catch aflight to Atlanta, GA, to attempt an observation.Just before boarding the flight, I called Joan; sheread me some observations which Arnold Klemola hadjust phoned from Lick Observatory. Three exposureshad been taken on Sept. 11, but the plate measure-ments could not be reduced earlier due to computerproblems. I had known about the observations andhad computed a list of topocentric positions, whichI had with me. Using a pocket calculator during theflight, I computed the paths from Klemola's data.Two were in good agreement with the Lowell results,but the third path was over an arc second farthersouth. In any case, Atlanta was near the center ofthe predicted path, and I only had time to drive toRiverdale, a suburb just far enough south of thecity to avoid serious light pollution. The occulta-tion lasted 134 seconds. I timed a "probable blink"a few seconds before the (main) disappearance. Ag-laia seemed a little brighter than predicted, sinceI could see it with njy 20-cm telescope during theoccultation.

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Around Atlanta many miles north and south of River-dale, R. Wi11iamon at Fernbank Science Center and H.Landis at Locust Grove photoelectrically recordedthe occultation. Of the three Lowell stations, onewas clouded out, one had a miss, and the other re-corded the occultation. Several other chords wereobtained near Phoenix to south of Tucson, AZ, in-cluding an image-intensified video record by PeterManly. Ben Hudgens timed a X-second occultation atClinton, MS, apparently near the southern limit.Roger Harvey saw no occultation at Concord, NG, ap-parently the American closest to the northern limitto see a miss (he saw Aglaja approach the star, cen-trally as well as he could tell. Bob Melvin reportsthat several others in the Carolinas were cloudedout.

Unfortunately, it was cloudy over much of the pathin Texas. But Paul Maley found a large clearing atMt. Enterprise, and saw a miss. At a location 5miles farther north, Chuck Herold timed two briefoccultations of the star, the first lasting two sec-onds and the other lasting only 0.5 seconds starting0.7 second after the first reappearance. The firstdisappearance was gradual, lasting a full second.Chuck said the star turned red as it faded. Wasser-man's preliminary analysis gives a smaller-than-pre-dicted diameter of about 135 km for Aglaja, and itshows that Chuck Herold's site was near the southernlimit of the occultation. But his timings disagreeby about half a minute with the other timings of theevent, and the discrepancy still is being investi-gated.

Was the extreme accuracy of the prediction from thenew Lowell telescope a fluke, attributable to begin-ner's luck? I think not. The telescope character-istics are similar to those of the Lick astrograph.These two astrographs are the only ones with a gen-erous plate scale and with a large-enough field sothat only the accurate Perth70 and AGK3R referencestars are needed for the plate solutions. The sta-tistics from large numbers of exposures measured au-tomatically (and therefore accurately) virtuallyguarantees accuracies much less than 0!'1. The onlyastrometric observations of known comparable accura-cy for asteroid events have come from very long-fo-cus smaller-field telescopes where secondary starpositions measured from Lick plates were used forthe local plate reductions; and from the photoelec-tric transit telescope at Bordeaux, France (see page168 of the last issue). The positions of SAD andAGK3 stars are often now in error by an arc secondor more, and are often systematically in error withdiscontinuities near the edges of the plates usedfor the Yale and AG catalogs. For asteroid occulta-tion astrometry, this often results in errors of 0!'5or more, even though the internal accuracy of 3 or 4exposures may be much less. At the moment, it isnot possible to assess the accuracy of plates takenwith the Astrographic Catalog camera at the Cape Ob-servatory. Secondary star positions reduced fromwide-field plates (taken with another telescope atCape) using accurate data from the Southern Refer-ence Star rogram (SRS; the Perth70 catalog is partof the SRS¶ have been used. None of the occulta-

tions predicted with astrometry from this telescopehave been observed due to bad luck with weather andthe paths often ending up over the ocean.

1Ae all hope for a long and productive future for thenew Lowell astrographic telescope. It is now some-

what difficult to use, with a wooden plateholder andPlexiglass filter slide. The success with Aglajacertainly shows that it deserves better accessoriesto facilitate routine use. Robert Mi11is plans topresent preliminary results from the September 16thoccultation at the meeting of the American Astronom-ical Society's Division of Planetary Science inKona, Hawaii, this month, and it will certainly alsobe mentioned at the IOTA meeting in Houston on the20th.

ASTEROIDS AND THE GRAVITATIONAL CONSTANT

David W. Dunham

Articles about the gravitational constant derivedfrom analysis of the very accurate range measure-ments to the Viking landers on Mars have been pub-lished in o.n. 3 (6), 118 and p. 158 of the last is-sue. An article, "Determining Asteroid Masses fromPerturbations on Mars," by J. G. Williams, Icarus 57(I), I, sheds more light on the matter, and urgesthat good diameters be determined from occultationobservations of several asteroids which affect Mars'orbit the most.

Williams notes that determination of Gig to accura-cies better than 1q"11 from the Viking data requiressolving for improved masses for the three largestasteroids and good modeling for the accelerationsdue to the smaller ones. There is some controversyover the best way to do this. Although the accuracyof the result by He11ings et al. given in o.n. 3 (6)was 0.4 x 1q"11, an accuracy of 3 X 10"1! using adifferent asteroidal model is given for GIG by R.Reasenberg in "The Constancy of G and Other Gravita-tional Experiments" in philos. Trans. Roy. Soc. PartA, in press when Williams' article was published.Reasenberg's uncertainty is a little larger thanthat from lunar occultations given in can. 3 (8) 158.

Williams describes how the masses of the outer plan-ets can be improved from analysis of the Viking da-ta. The data also are sensitive to more distant ob-jects which have been the subject of speculationduring recent years. Williams says that the currentanalyses of the Viking data rule out the possibilityof an undiscovered planet as large as the earth to adistance of about 100A.U., and of a star as massiveas the sun to a distance of about 40,000 A.U.

Williams states, "If future missions to Mars are tohave the capability of testing GIG at levels belowabout 0.3 x 1q"11, it will be necessary to improveon our present knowledge of asteroidal densities anddiameters." He stresses that physical information,especially accurate diameters, be determined for allof the asteroids in Table III of his paper, noting:"Clearly, the objects of the table are prime targetsfor occultations." The asteroids in Table Ill havethe following numbers: 1, 2, 3, 4, 6, 7, 8, 9, 10,13, 14, 15, 16, 18, 19, 20, 22, 24, 29. 31, 41, 45,51, 52, 65, 78, 97, Ill, 324, 372, 405, 409, 511,532, 704, and 747.

OCCULTATIONS DURING TOTAL LUNAR ECLIPSES

David Herald, David W. Dunham, and Paul Maley

Herald has analyzed visual occultation timings madeduring the past five total lunar eclipses in Aus-tralia and New Zealand, as reported in Circular

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184

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C84/9 of the Occu1tation Section of the Royal AstronomicalSociety of New Zealand. Plots of the residuals as a func-tion of position angle show the best-fit sine curve repre-senting solutions for corrections to the lunar right as-cension (not longitude, as printed below the plots), dec-lination (not latitude), and radius. Actually, the radiusused by Herald in his calculations was O'J05 smaller thanthat usually used for occultation work, in good agreementwith the average radius correction of +O'j06 from all

^M^L.'Y'exg ow ogc^jl.t~txcj~so»=En%0'«xj DLJFQXMO "THE L.LJM^* EGL-XPSE CJF"

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eclipses. The plots for only the first threeare reproduced here. Those for the 1982eclipses will be published later, after Dunhamhas time to go through his records and sendHerald the numerous timings he has receivedfrom North Americans and others. A few obser-vations of the 1982 eclipses made in the So-viet Union were received recently. If thereare still some unreported observations of the1982 eclipses, please send them to Dunham atP.0. Box 7488, Silver Spring, MD 20907, U.S.A.He still has no reports from japan, and fewtimings from other observers in Asia. We hopethat when we publish the results for the 1982eclipses, we also can list all observers whocontributed, ranked according to the number ofvalid timings used in the solutions (with re-appearances weighted extra).

The plots show a concentration of observationsnear position angle 90° due to a paucity ofgraze data and reappearances. The scatter israther large due to visual timing, star posi-tion, and Watts limb correction errors. Thestar positions can be improved by good astro-metric observations, such as those made atLick Observatory of the 1982 eclipse fields.Timing errors could be eliminated by usingphotoelectric or image-intensified video ob-servations, and attempts using the latter areencouraged during future eclipses.

The next total lunar eclipse is on 1985 May4th, visible from the Eastern Hemisphere.Sometime before the eclipse, Dunham plans todistribute extended-coverage total occultationpredictions to observers there, but Astro-graphic Catalog star positions for the starfield in Libra need to be generated first.Herald can generate plate constants for theA.C. measurements with SAD data. Dunham canuse the plate constants to generate right as-censions and declinations of all the starsfrom the x-y measurements given in the A.C.We may need someone to volunteer to punch thex-y data for us, either on cards or to floppydisk (using a microcomputer; the data thencould be transferred to the IBM 4341 at USNO).

This eclipse will be unusual because 2.9-mag.Zubenelgenubi (Alpha Librae) will be occultedduring totality. This will not happen againfor 19 years (one Metonic cycle later, duringthe eclipse of 2004 May 4), according to G. P.Konnen and Jean Meeus in their article, "Qc-cultations of Bright Stars by the EclipsedMoon," j. Brit. Astron. Assn. 85 (I), 17(1974). The only other occultation of a starbrighter than mag. 3.9 by a totally eclipsedmoon before 2004 will be an occultation of3.5-mag. Delta Geminorum on 2001 January 9(during a small partial eclipse on 1994 May25, Beta Scorpii will be occulted by theeclipsed part of the moon for some areas).Zubenelgenubi is a triple star. 5.3-mag. Al-pha 2 Librae is about 3' away (this star it-self may be a close double). The magnitudesof the close components of Alpha 1 Librae are3.4 and 3.8; their separation likely variesdue to orbital motion, but was 0!'01 during aprevious occultation.

0

OF"

Correc¢6on to the Moon'w lon9i¢uqe " ".07: .IS

Correction to the Moon'6 l&CltuQ0 " .49: .20

Correction to tho P'kjqn'w red$u6 m -.OS: %13

185

~

IOTA'S plans for an expedition to observe the May4th eclpse have stalled due to other more urgentmatters. We would like to observe at the northernlimit of the graze of Zubenelgenubi; plans have beenmade to observe at the southern limit by members ofthe Astronomical Society of Southern Africa. Wewanted to observe from the Seychelles, but thenorthern limits of both Alpha 1 and 2 missed all theislands there. The paths also cross Algeria, Libya,the Sudan, Ethiopia, and Somalia, which all haveeither political or suitable mapping problems. Thepath for Alpha 2 Librae passes less than 10 km fromthe center of Addis Ababa and about 50 km to thesouthwest of that for Alpha I. The best possibilitymay be Alpha 1 about 50 km south of Khartoum, wherethere is a network of irrigation canals. Theeclpse will occur very high in the sky in the Sey-chelles. Unfortunately, no grazes of SAD starscross any of the accessible islands. The Alpha Lib-rae paths pass near some of the islands, but centralgraze is on the penumbra there, not in the umbraduring totality, as is the case for Africa. HansBode notes that it is possible to arrange trips fromthe German Federal Republic to the Seychelles, stay-ing for 2 weeks for DM 1500, all expenses included.Weather prospects and other information about theseareas still need to be determined. we are trying tocontact a member of the British Astronomical Associ-ation who recently observed a lunar occultation ofMars in the Sudan.

OBSERVATIONS OF ASTEROIDAL APPULSESAND OCCULTATIONS

Jim Stami

Observations of appulses and occultations of starsby asteroids should be sent to me at Route 13, Box109, London, KV 40741, U.S.A., telephone 606,864-7763. Send a copy of the report to David Dunham,P.0. Box 7488, Silver Spring, MD 20907, U.S.A., onlyif an occultation has been observed which could usesome analysis for comparison with others, and indi-cate to whom copies have been sent on the report.Dunham prefers not to have to send me copies of num-erous reports sent only to him. Alternatively, youcan send your report to a local or regional coordi-nator who then can send the results on to me. Euro-peans can send their reports to R. Boninsegna; Ruedc Mariembourg, 33; 6381 Dourbes, Belgium; he hasbeen sending good sumary reports to us. In the ac-counts of individual events below, a reference to aprevious preliminary o.n. account of the event, ifany, is given in parentheses following the date.

(9) Metis and SAD 184440, 1981 jun 14: An occulta-tion was observed photoelectrically in the USSR ac-cording to L. Kristensen in his article about theFebruary 19, 1984 event discussed below.

(106) Dione and SAD 80228, 1983 jan 19: (O.N. 3 (S)104). From Astron. Nachr. 305 (4), 207-211 (1984);Final results from the data of 12 amateur astrono-mers and one professional in Denmark, Gemany, andthe Netherlands show this asteroid to be egg shapedwith a mean diameter of 147 ±3 km. Final results,computed by L. Kristensen.

(683) Lanzia and SAD 117317, Nov. S: J. Pinson, us-ing a 35-cm telescope at La Seyne-sur-Mer, France,saw no occultation between 5h30m and 5hSOm U.T.,while G. Leonis and L. Zhmermann used a IO-cm at

Charneusc, Belgium, to record a negative observationfrom 5 39 50 to 5 49 50 .

(199) Byblis and SAD 78120, Nov. 20: Under cloudyskies, j. F. Petrucci and T. Lesnes managed to ob-serve from 5h18m to 5h21m, 5h23m to 5h28m, and 5h33mto 5h35m, with a 30-cm scope at Hyeres, France,without detecting any occultation.

(1467) Mashona and AGK3 +50°0390, Dec s: No occul-tation was observed from about 20h45m to 21h04m byR. Boninsegna with a 30-cm at Dourbes, Belgium, andfrom 4 French stations: Dubois and Florsch Halbnachswith a 49-cm at Strasbourg Observatory, j. Pinsonwith a 35-cm at Seyne-sur-Mer, B. Candela with a 20-cm at Lo11ies-Pont, and j. F. Petrucci with T.Lesnes using a 30-cm at Hyeres.

(208) Lacrimosa and SAD 78799, Dec 14: J. Aloy atBarcelona, Spain (o.n. 3 (8), 168), and 7 stationsin Belgium all reported no occultation from about23h20m to 23h40m: j. Bourgeois with a 25-cm at Fur-fooz, G. Leonis with a 25-cm at Uccle Observatory,A. Sorro and L. Zimerman with a 28-cm at Brussels,P. Poitevin with a 25-cm at Herk-de-Stad, P. VanCauteren with a 25-cm at Aartsclaar, A. Lheureusc,Y. Thirionet, and M. Decominck with 15- and 20-cmscopes at Brussels, and C. Bactens at Boechout.

(91) Aegina and SAD 76615, 1983 Dec 30: Twelve sta-tions reported on this event, with the only probableoccultation (80% certainty) being observed by D.Barbany at Grano11ess, Spain. Using an B-cm instru-ment, he timed a l-sec. extinction at 22h56m43s.Others reporting timings from Belgium were P. Louisand R. Boninsegna with 30 cm at Dourbes (22h40m to23hOOn30s), A. Worm with 16 cm at Brussels (22h40mto 23hOOm), and C. Kint and G. Leonis at Uccle Ob-servatory 22h40m39s - 22h47m and 22h49m43s -23hOim49S). L. Louys monitored from 22h45m to 23hOOm with50 cm at Tenerife in the Canary Islands. French ob-servers incjuded L. Bellotto with 30 cm at La Seyne-sur-Mer (22 30m - 23h05m), B. Candela at Lollies-Pont using 20 cm (22h30m - 23hOSm), T. Lesnes atHyeres with 30 cm (22h3P - 23hOim), and j. F. Le-borgne with 16 cm at Brest (22h44m - 23hON).

(154) Bertha and 13 mag. star-, 1984 jan 12: P.Poitevin used a 25-cm telescope from 18hOOm to 18hO2m at Herk-de-Stad, Belgium, to monitor the star,but there was no event, and it clouded up after twominutes of observing, according to a report of Euro-pean observations received from R. Boninsegna.

(194) Prokne and SAD 117122, jan 20: (O.N. 3 (8)168). At London, KV, I monitored the star from 6hSSm to 7h13M5s with a 20-cm SC, observing no ex-tinctions Ion er than 055, except for a 155 loss ofthe star at 7hgogn45s, probably due to fatigue, a

warm scope, and -21° C temperature. Michael Grist,at Burns, TN, had clouds as well as -16" C tempera-ture to hinder his observations with a 36-cm SC. Hemonitored from 7hOyn to 7hRm with breaks at 7h07m19S to 7h07tn42s and 7hlOm37s to 7h10M4s. BennyRoberts and Ben Hudgens, using 33-cm and 25-cm New-tonians, respectively, saw no events from 6hSSm to7h20m at Jackson, MS.

(41) Daphne and SAD 112434, jan 26: R. Burchi, A.DI Paoloantoni, et al, at Teramo, Italy, monitoredthe star with photometers from jgh to 20h, with noextinction, while 5 other astronomers in Belgium al-

186

so recorded no occultation: L. Zimermann at Brus-sels with a 16-cm refractor (18h2U to 18h3¥), G.Leonis at Brussels using 28 cm (18hlP05s to 18h3%)21S), p. Poitevin with 25 cm at Herk-de-Stad (18h31mto 18h40m), F. Van Sod (18h2&n to 18h42m) with 25 cmat Wagem, and P. Van Eauteren (18h2¥30s to 18h41m)with 25 cm at Aartsclaar.

(46) Hestia and AGK3 +3°1471, jan 29: (O.N. 3 (81,

168). C. Gualdoni and M. Cavagna observed from 414m to 4htiSm with no event detected at M. Bornia,Italy. j. F. Leborgne at Toulouse, France, used a20-cm from 4h16m to 4h4¥ with no occultation ob-served. A. Maury monitored the star at Grasse,France, with a refractor and photometers from 4h2Pto 4h47m and 4h47m to 5hOlm without any extinctions.Also no occultation was seen in France by B. Candelaat Lo11ies-Pont, T. Lesnes at Hyeres, D. Bockeleeand j. Lecacheux with photometers at Haute-ProvenceObservatory, and j. Pinson at Seyne-sur-Mer; and byA. Estela and J. Fabregat at Valencia, Spain.

(194) prokne and 12.2 mag. star, jan 30: FerruccioGine11i observed a 1352 extinction beginning at 22h2P37S U.T.C., from Fortaleza, Brazil. He used a32-cm Newtonian under good skies, and was sure ofthe event. This observation shows a shift of 0!'8north, placing the path also over southwest SouthAfrica, but no reports of this event have been re-ceived from there yet. This is the first observa-tion of an asteroidal occultation of an AstrographicCatalog star not in the SAD or AGK3.

(12) Victoria and 11.8 mag. star, Feb IS: I moni-tored the star with an B-inch SC from Oh4P to 1h02m

at London, KV. No event was detected, in less thanaverage seeing. After significant separation at jhjgn, Victoria seemed brighter than the star.

(9) Metis and SAD 119464, Feb. 19: (O.N. 3 (8).168). The chords of observers at Bech, Larsen,Klinting, Aarhus, and Esbjerg, Denmark, and at Kieland Liibeck, German Federal Republic are plotted byKristensen in Astronomi & Rumfart, May-june 1984, p.76. He fitted the data with a 170-km by 210-km el-lipse. Wolfgang Beisker also noted that the Liibeckobservation was photoelectric, and gave details forvisual timings made at Rathe and Kalauc, German Dem-ocratic Republic. A. Figer at Paris monitored thestar from 1h2Sm to 1h42m with a 26-cm scope withoutobserving an occultation. R. koninsegna used a 30-cm at Dourbes, Belgiwb from 1 2P2QS to 1h41m with-out observing an occultation greater than 1 secondin length.

(9) Metis and BD +8°2579, Mar IS: (O.N. 3 (8) 169).S. Maksymnire observed from 4hlOm to 4h3(yn with anll-cm instrument, without an event, from Asernes,just north of Conde-sur-Noireau, France.

(114) Kassandra and SRO 169989, Mar 23: Buffet Maz-alrey, using a 28-cm scope at Vernon, France, ob-served no occultation from 4h23m to 4h 43'L P. Ba-rufetti at Massa, Italy, saw no event from 4hom9sto 4h41m44s with a 31-cm glass.

(324) Bamberga and 12.3 mag. star, Apr. 3: PeterAnderson observed from Brisbane, Australia, and re-ports that the asteroid seemed to merge with thestar 10 minutes later than the predicted time.

(128) Nemesis and SAD 139402, May 2: Six members of

the Southern Cross Astronomical Society reported a"no event" for this event. M. C. Mooney used a 36- .cm SC, and R. Scott Ireland used BO-m binocularsfrom 1h35m to 1hSOm, at the Southern Cross Observa-tory. The other 4 members, spread around Dade County, FL, were R. Riefes (1h31m to 1h45m), W. T. Doug· tlas (lh3¥ to lh45m), Don Parker (1h31m to lh49m),and R. Grant (1h35m to 1hSlm). jose Izaguirre andDomingo Sanchez, observing in Venezuela with lS-cmand ZS-cm telesco es, respectively, reported no qc-cultations from OfOOn to 2h40A Observations with

the Bordeaux transit telescope over several nights ·from Apr 11 to 26 showed a south shift of O'A9±O:'I2.and a time shift of 2.2 ±0.5 minutes early. Thisplaced the path over southern Brazil and the southcoast of South Africa.

(230) Athamantis and SAD 158162, May ii: Observa-tions at Bickley Observatory in Perth, Australia, onMay 9 showed a one arcsecond south shift, placingthe path between Sydney and Canberra. These updateswere phoned to a number of coordinators, includingPeter Anderson in Brisbane, resulting in nine sta-tions that monitored the event visually. Four ofthe stations obtained positive results: S. J.Hutcheon, J. Cali and G. Bond, T. and D. Hickey, andP. E. Anderson. The chords obtained give a roughidea of the size and shape of the asteroid. The re-sults are detailed in Circular C84/6, the April 1984publication of the Occultation Section of the RoyalAstronomical Society of New Zealand, from which thediagram is reproduced.

NORTH

m

,],0~ The longest chord was- 130 km, longer than

t - the predicted mean- diameter of 116 km.

f£

I 8econd

f EAST

_1,'i" \' ' ' '"""",:, >\\ —\ -"" \

O O

-LO AD

Diagram basedupon calculationsby. D. Herald.Units are 1/1000of the earth's radius.

4.,,:i:%:%>

(326) Tamara and SAD 226130, May is: Based onplates obtained by joe Chums at Cape Observatory,South Africa, on May 10, a shift of 2'26 north and1.9 minutes early (mostly due to the asteroid ephem-eris) was predicted by David Dunham. This wouldplace the path over southern Chile, central Argenti-na, central Africa, and southern Saudi Arabia.

187

(21) Lutetia and SAD 158714, May 16: Arnold Klemolaobtained plates for this event on Apr 24, and Dunhamsent updated predictions to Mexico, Hawaii, and Ja-pan; predicting a shift of 0':48 north ±0!'15, and 1.5minutes late ±0.3 minute.

(19) Fortuna and 12.0 mag. star, May 25: Peter An-derson, observing from Brisbane, writes that the as-teroid seemed brighter than the star.

(326) Tamara and SAD 225520, jun 2: Chums obtainedplates on May 28. Because of the May 30 eclipse,

Dunham was not able to compute shifts until afterthe event, so there was no notification. In anycase, the resulting 3!'0 north shift, due primarilyto the error of Tamara's ephmeris, took the path ofthe event off the earth's surface. Likewise, theJun 4 occultation of SAD 225478 by the same asteroidalmost certainly missed the earth.

(602) Marianna and SAD 227909, jun 2: The sameplates and computation as mentioned above gave a 2!'5;outh shift, placing the path south of South Africa,but possibly catching the southern part of New Zea-land. C. Frick, at Com, Australia, and C. Bem-brick, at Queenscliffe, Australia, observed the ap-pulse, with no occultation occurring.

(624) Hektor and AGK3 +7°46, jun 2: C. Bembrick al-so observed this event without seeing an occultaticn.

(386) Siegena and AGK3 +5°2112 jul 16: Marco Ca-vagna observed from Oh20m to Oh44m near Como, Italy,

with a 25-cm reflector, seeing no occultation.

(110) Lydia and SAD 211065, jul ib: B. Loader, atBlenheim, New Zealand, S. G. Ryan, at Christchurch,N. Z., and P. E. Anderson, at Brisbane, Australia,all report no extinction for this event.

(94) Aurora and SAD 211730, jul 28: Australian ob-servers S. J. Hutcheon at Sheldon, and P. E. Ander-son at Brisbane, observed this appulse without ~t.

(451) Patientia and L 931708, Aug s: P. E. Andersonobserved at Brisbane, but saw no occultation.

704) rnterainnia and L 944324, Aug s: jim Young, at"iable Mountain Observatory in California, photoelec-

trica11y recorded a 10% drop with a 61-cm telescopefrom 6h41m45s to 6h42mm)2s. Plates taken at Lick Ob-servatory were analyzed at Lowe17 Observatory, andyielded a south shift of 0!'7 and a time shift of 1.5minutes early, placing the path over Los Angeles andmost of southern California. The observation showedthe event to be 1.0 minute early. At. Mt. JOhn,N. Z., A. C. Gilmore and M. Clark monitored the starwithout detecting any event.

(704) rnteramnia and l 941608, Aug 8: On Aug 5,Klemola obtained plates, and a telegram was sent toGraham Blow in New Zealand, since the predicted pathwould cross New Zealand and southeast Australia.However, the low magnitude drop for this event pre-vented most of the potential observers from gettingany results.

(87) Sylvia and SAD 211985, Aug 8: Astrometry byChums on Aug 6.9 led to a predicted shift of 2':14south ±0!'2 and 5.2 minutes late ±0.5 minute. Dunhamtelephoned Blow 6 or 7 hours early, and Blow relayedthe astrometry to several observers. Mike Clark at

Mt. John Observatory monitored photoelectricallyfrom 17h43m to 17h5P, while Carlsson Chambliss andjim Bruton at Black Birch did the same from 17h27mto 18h24m. No events were recorded. Several otherphoto-monitor attempts were unsuccessful due toequiµnent and the bright background problems. SteveHutcheon in Queensland confirmed that the planetseemed to have passed south of the star. Others ob-serving from New Zealand were S. G. Ryan and L. Hus-sey (Christchurch), G. L. Blow and J. Priestley(Wellington), and R. R. D. Austin (New Plymouth).P. E. Anderson also monitored at Brisbane. [Noteadded early October:] M. D. Overbeek tells us thata R-second occultation was reported by an observerin Port Elizabeth, South Africa, 4 minutes laterthan the nominal time. The observer did not knowabout the astrometry. The observation is consistentwith the time from the astrometry, but the impliedpath is 0.3 arc second north, which would pass en-tirely north of Australia. Graham Blow reports thatPeter Anderson, at Brisbane, Australia, believedSylvia passed north of the star at his location,which is consistent with an occultation at PortElizabeth. Since the predicted central duration was24 seconds assuming a diameter of 275 km, Port Eliz-abeth probably was close to one of the occultationlimits.

(SI) Nemausa and 12.3 mag. star, Aug IS: P. E. An-derson observed this appulse from Brisbane withoutany occultation occurring.

(704) Interamnia and L 941618, Aug 19: K1emola gotplates in early August showing a path shift to cen-tral Texas, the western plains, and up to Saskatche-wan. This was, however, another low magnitude drop,and no observations have been reported.

(104) Klyinene and SAD 185260, Aug 25: R. R. D. Aus-tin at Plymouth, N. Z. saw no event during this ap-

pulse.

(704) Tnteramnia and L 941624, Aug 29: Klemo1a'searly August plates showed a path through Patagonia,off the coast of Chile, and southern Peru. Also alow magnitude drop.

(747) winchester and BD +4°978, Sep 2: Under excel-lent skies, Benny Roberts at jackson, MS, with a 33-cm Newtonian; Tony Frewan just east of Prinevi11e,OR, with a 20-cm SC; and I, at London, KV, with a20-cm SC, all obtained negative observations. I be-gan monitoring at 1Ohl> when I still could see sep-aration, and watched the asteroid skim the northerned e of the star with 120 power. Roberts began atio8ocm, and watched the asteroid approach, merge,

and recede, until 10h29, with 125 power. Fremanused 111 power, and detected Winchester about 3 arcseconds due east at 10hocm. He was unable to tellwhether the asteroid passed north or south of thestar, qnd observed until 10h2N.

(704) Interamnia and BD -19 4924, Sep 2: K1emola°searly August plates indicated a path through westernIndia and western China, and Lowell Observatory senttelegrams to Uttar Pradesh State Observatory on Man-ora" Peak, Naini Ta1, and to Kovalur Observatory,Bangalore, India, since there was a good drop inmagnitude for this event.

(209) Dido and SAD 188498, Sep 4: Plates obtainedby Kl«no1a on Aug 27 led to a predicted shift of 2'!0

1~"

188

SW ±0'.'3, and 10 minutes late ±2 minutes, while as- IOTA GRAZING OCCULTATION MAPStrometry by Chums led to a predicted shift of 2':9west, and 9 minutes late. The main reason for the David W. Dunhamlarge shift was an error in the declination of thestar. The path was shifted to the Pacific Ocean in I have set up a system to produce maps of the north-daylight. ern and southern limits of occultations using the

same USNO input data used by the computors to gen-GRAZES. 1984 JULY 20 TO DECEMBER 31 crate IOTA'S detailed grazing occultation predic-

tions. The Meeusmap program, which is being dis-

4Si3 tributed to all of the computors along with the3t · graze input data for 1985, generates a magnetic

tape containing the path data for specified input

* longitude and latitude boundaries. The magnetictape is read by my Grazemap program which actually

<?k , i - " ' i . produces the plot, including asterisks at stationsL _A" whose longitudes and latitudes are specified. AnA _ example is shown at left, covering most of theT b * northeastern part of the U.S.A. and including 36grazes of stars brighter than mag. 8.1 from lateI i i i . July to the end of this year. Time tick marks, atT - . B integral Z-minute intervals of Universal Time, areU " on the north side of southern limits and are southD ' " of northern limits, that is, on the side where aE * total occultation occurs. Grazes on the dark limb

k ?Aare drawn as s lid line , and those on the sunlit

* side are dashed lines. Graze paths end with A" (altitude too low), S (twilight too bright), and B3E; zzi (bright side interferes), if they do not go to the

^ F edge of the map. The maps produced by Grazemap* I are false projections, where both the longitude

_85" -75 -70° and latitude scales are linear (the longitudescale is compressed relative to the latitude scale

LONGITUDE by the cosine of the latitude of the map center).Hence, it is rela-NO. YEAR MO DAY USNO # SAD MAG. STAR NAME PLACE D % SUNL LIMIT W.U.T. tively easy to plot

the position of a1 S 1984 JUL 21 300 110295 7.8 KV-Ont. V 48 WAN NORTH 9h32"0 location whose Ion-2 1984 JUL 23 517 93494 6.4 26 B. TAURI TN-ME 29 WAN NORTH 7 12:2 gitude and latitude3 1984 JUL 24 X5728 76609 7.5 TN-ME J 20 WAN NORTH 7 07.5 are known, or to4 1984 JUL 24 665 76618 5.7 247 B. TAURI TN-ME U 20 WAN NORTH 7 50.7 measure the coordi-5 1984 AUG 18 372 92991 7. 6 KY-Que. 64 WAN NORTH 9 22.5 nates of a point on6 1984 AUG 19 X4181 93331 7.6 TN-MA 56 WAN NORTH 4 32.2 thC map. An index7 1984 AUG 21 X6335 76853 7.7 VA-DE 35 WAN NORTH 5 16.1 number in the mid-9 S 1984 AUG 22 X8235 77932 8.0 NG 24 WAN NORTH 10 05.1 die of the track

11 1984 SEP 3 2459 185049 7.2 MI-ME 56 WAX NORTH 0 49.6 identifies the12 1984 SEP 22 1435 98742 6.6 57 B. LEONIS IN-ME 11 WAN NORTH 9 42.4 graze in the table.13 1984 SEP 29 X21720 183833 7.8 KY-PA 20 WAX NORTH 0 30.214 1984 OCT 1 2558 185779 6.2 4 G. SAGITTARII IN-Que. 41 WAX SOUTH I 06.5 Most of the colwm15 1984 OCT 2 2721 187239 3.3 PHI SAGITTARII SC-YA X 51 WAX NORTH 0 17.9 headings of the ta-16 1984 OCT 2 2723 187246 6.7 SC-YA 51 WAX SOUTH 0 28.8 ble are self-ex-18 S 1984 OCT 4 X29678 190337 7.3 L.ERIE-ME 79 WAX NORTH 23 12.7 planatory. The19 1984 OCT 13 531 93557 5.5 13 TAURI IN-NJ V 90 WAN NORTH 10 41.7 star's double Star20 1984 OCT 14 634 76551 5.3 56 TAURI KY-VT 85 WAN NORTH 2 00.1 code is given under21 1984 OCT ]4 656 76601 4.4 KAPPA TAURI MI V 84 WAN NORTH 5 07.3 "D," and the sunlit23 1984 OCT 17 X10949 79316 7.9 IN-MA 55 WAN NORTH 8 25.5 percent of the moon24 1984 OCT 19 1373 80702 6.1 90 HI. CANCRI NC 34 WAN NORTH 5 46.9 is given under "%25 1984 OCT 21 X16870 99505 7.9 IN-L.I. 14 WAN NORTH 8 52.0 SUNL." "W.U.T." is26 1984 NOV 2 3242 0 7.8 KY-ME 65 WAX SOUTH 4 15.4 the Universal Time27 1984 NOV 4 3480 146799 7.3 352 B. AQUARII TN-Que. 81 WAX SOUTH 1 55.6 of central graze29 1984 NOV 11 742 76858 6.0 99 TAURI NC-ME A 95 WAN NORTH 1 02.3 at the westernmost30 1984 NOV 12 900 77775 4.9 139 TAURI Ml-Ont. 89 WAN NORTH 3 07.1 point of the path32 1984 NOV 14 1211 79869 6.2 4 CANCRI Ml-Ont. C 71 WAN NORTH 6 24.0 on the map. On33 1984 NOV 20 X19474 139403 6.0 S VIRGINIS 9 WAN SOUTH 9 13.7 this map, there was34 S 1984 NOV 20 1951 139447 7.1 81 VIRGINIS MI-NJ M 8 WAN SOUTH 11 32.2 a program error35 S 1984 NOV 24 2575 185900 6.8 11 B. SAGITTARII Ml-Ont. K 5 WAX SOUTH 22 16.6 which resulted in36 1984 NOV 26 2910 188722 4.8 OMEGA SAGITTARII ATLANTIC 18 WAX SOUTH 23 07.0 "B" being written37 1984 NOV 26 X27771 188749 8.0 NC-VA 19 WAX SOUTH 23 49.3 at the ends of38 1984 NOV 27 2914 188778 5.0 60 SAGITTARII 1N-Ont. V 19 WAX SOUTH 0 31.7 paths with bright39 1984 NOV 27 3052 189801 6.4 86 B. CAPRICORNI MI M 27 WAX SOUTH 23 33.0 twilight, instead40 1984 NOV 29 X30071 164654 7.9 ATLANTIC 37 WAX SOUTH 1 58.8 of "S." An "S" has41 1984 DEC 14 X15882 99202 7.7 MI-MA 65 WAN SOUTH 6 14.8 been written be-42 1984 DEC 18 X20068 158405 7.5 VT-ME 19 WAN SOUTH 10 57.1 tween the number

_

189

~

and date in the table for these cases. The "PLACE"column was written in manually to identify thestates (by two-letter postal abbreviations) and Can-adian provinces in which the western and easternends of the graze paths on the map are located.Grazes in the tape generated by the Meeusmap programcan be removed from the plot by specifying theirnumber in a "deletion list" input for the Grazemapprogram. This has been done for 6 grazes in the ex-ample, because they only crossed ocean or occurredunder quite unfavorable conditions in the area ofthe map. The information needed to select whichgrazes to reject is available in the printed outputfrom the Meeusmap program. I plan to add a more so-phisticated observability rejection code whichshould minimize the need for manual deletion. If alimit for a bright star passes only over the ocean,it may be useful to keep it if a total occultationis visible from land, as a reminder and to help es-timate the circumstances at various locations.

This map is reproduced only as an example. Sincethese maps are primarily of only local interest, Ido not intend to publish them regularly in o.n. Themap here was distributed with information aboutplanned expeditions from the Washington, DC, area toabout 150 observers, most of them in the Mid-Atlan-tic states and most of whom have participated inpast expeditions which I have organized. I alsosend these notices to most IOTA members in the re-gion shown, but not to some, especially in the morenorthern and western areas of the map. If you wantto receive my semiannual expedition mailings, whichnow will include these graze maps, write to me atP.0. Box 7488, Silver Spring, MD 20907.

For future maps, I plan to correct the "B" errornoted above, and probably will limit thw to 25paths Or less (for maps covering a region of thissize) to reduce clutter. I plan to rearrange thetable, adding some information, yet making it morecompact. The stations shown on the map are observa-tories with photoelectric capabilities (except forCape Hatteras); in the future, I plan to plot in-stead the stations for those receiving the detailedgraze predictions. Similar maps can be produced forother parts of the world. However, our resourcesare limited, so I do not want to duplicate maps be-ing produced by the ILOC. The IOTA maps are intend-ed primarily for regional publications. If you areinterested in including such maps in a regional pub-lication, contact the computor who normally sendsyou the detailed IOTA graze predictions, specifyingthe faintest magnitude wanted, the desired mapboundaries, and stations for which asterisks shouldbe plotted. Try to request maps at least two monthsbefore they need to be sent to the publisher. Ifpossible, maps should be included entirely withinone of the 1000-mile-wide "super standard station"prediction regions which have been assigned lettersand are used for the graze predictions generated atUSNO. At present, if a map for a larger region iswanted, the graze data for the different superstandard station regions have to be merged manuallybefore being input to the Meeusmap program. Thiswas actually done for the first IOTA graze map whichI produced, the one of the contiguous states of theU.S.A. published On pages 52 and 53 of this month'sissue of Astronomy magazine. In that case, themerging was not a large job, since only relativelybright stars were selected.

The database of physical and political boundarieswhich I use for these maps is the same as that usedfor the regional maps for asteroidal occultationspublished in o.n. It is too coarse for maps withscales expanded much more than the example shownhere. Unfortunately, the database does not includethe boundaries of the provinces of Canada, thestates of Australia, nor the republics of the SovietUnion. I know the format of the database, and withsome trouble, can update it. I hope to obtain thecoordinates of the boundaries of the Canadian prov-inces from the National Heather Service, since theyinclude them on their gridded geosynchronous satel-lite weather photoes.

The Meeusmap program gets its name from the methodit uses to compute grazes, by calculating the lati-tude and time for a series of equally spaced longi-tudes, which has advantages for producing paths tobe plotted on maps. This method was developed byjean Meeus and published in his 1967 article, "Lecalcul des occultations rasantes," Ciel et Terre 83(I), 3. I programed the method over a dozen yearsago, and Berton Stevens modified my program to readthe USNO graze data and generate IOTA-format predic-tions. My Meeusmap program is a further modifica-tion of Stevens' version. Rather than giving TANZ,its tabular output lists sin(0) x TANZ, which is thedimensionless elevation factor by which heightsabove sea level must be multiplied to tell how farnorth or south the sea-level limit given in the pre-dictions must be shifted in the direction perpendic-ular to itself. The factor is negative if the pathis to be shifted southward, which is the case formost grazes in northern temperate latitudes.

FORMAT ERROR IN USNO TOTAL OCCULTATION PREDICTIONS

David kl. Dunham

A new printer for the IBM 4341 computer at the U.S.Naval Observatory was installed in September, in themiddle of the computer runs which generated the 1985USNO total occultation predictions. Unknown to Ma-rie Lukac and me at the time, some of the formatstatements which originally were keypunched with BCDkeypunch machines result in some incorrect charac-ters being printed by the new printer. Specifical-ly, in the GRAZING OCCULTATION NEARBY and VARIABLESTAR messages in the USNO total occultation predic-tions, "#" should be "=" and "%" should be "(."With the new printer, a typical "graze nearby" form-ula prints as follows:

LAT. # 30.50 - 0.68%WEST LONG. - 95.15),

which doesn't make any sense; it should be

LAT. = 30.50 - 0.68(WEST LONG. - 95.15),

which is the way it printed with the old printer.Similarly, the "#" following "MINIMUM MAGNITUDE" inthe variable star message should be "=." We don'tremwber exactly where in the 1985 predictions theprinter change was made, but think that all of thepredictions for overseas observers, and for those inregions XB and XR, as well as some of the NorthAmerican observers (especially those with addressregion codes at the beginning of the alphabet, par-ticularly A and g), were printed with the old print-er and are all right. But other North American pre- .dictions were printed with the new printer and in-clude the error, which was first pointed out to meby Don Stockbauer in the E region (address code

190

AE230). Marie Lukac and I will soon try to changethe program so that the correct characters printwith the new printer.

The "graze nearby" messages giving the linear formu-la for the limit normally are printed only if thelimit passes within 3 miles of the location forwhich the predictions are computed. However, if thethird option is 4 (extended graze option), the mes-sage is printed for all limits which pass within 40miles of the station, and if it is 6, the radius isextended to 60 miles. The specific calculation isfor the distance of a line from the observer to thestar above or below the moon's surface at the timeof closest approach to the center, this distance be-ing .003. .040, and .060 lunar radii for standardoption, option 4, and option 6, respectively.Hence, projection onto the earth's surface can givethe message for much greater distances from the sta-tion. The four option numbers are printed to theleft of the address code on the top of each page;the first option is the minimum observability codeincluded in the predictions.

LAST-MINUTE ADDENDUM TO IOTA NEWS

David W. Dunham

The IOTA meeting was held on October 20, as planned.Chuck Herold's report about the meeting will appearnext time.

Although this issue contains a couple of articlesabout grazes, an article sumarizing expedition re-sults again has had to be postponed. We hope thatit will appear in the next issue, about a month from

now. Recent observations of northern-limit grazesfavor the 78A prediction version, which is used for

generating the profiles, but observers are cautionedthat even many bright stars currently have errors ofHi second of arc or more in declination.

LAST-MINUTE ADDENDUM - CHARGE CARDS

The IOTA Board of Directors has approved the charge-card arrangement (see p. IBO) conditional only onour not having to pay more than a nominal annual feein addition to the standard 4% charge on purchases.Our banker assures us that as we will be using ourown typewriter rather than renting an imprinter,there will be no additional charges. You now mayuse your VISA or MasterCard for payments to IOTA ifyou find that to be to your advantage; when youwrite, specify which card you are using, and includeyour signature and all the information in the raisedlettering. Card users must pay the full prices,which are shown below, followed by the discountprices in brackets for the use of those paying bycash, check, or money order.

o.n.'s price is $1.44[1.40]/issue, or $5.72[5.50]/year (4 issues) including first class surface mail-ing. Back issues through vol. 2, No. 13 still arepriced at only $1.04[1.00]/issue; later issues @$1.46[1.40]. Air mail shipment of o.n. back issuesand subscriptions, if desired, is 47¢[45¢]/issue($1.87[1.80]/year) extra, outside the U.S.A., Cana-da, and Mexico. IOTA membership, subscription in-cluded, is $11.44[11.00]/year for residents of NorthAmerica (including Mexico) and $16.64[16.00] forothers, to cover costs of overseas air mail. ForIOTA members, graze predictions and the photoelec-tric Supplanent are available without extra charge;non-manbers pay $2.08[2.00]/graze prediction, and$1.04[1.00] for the photoelectric Supplement.

'\

OBSERVED PROFILES OF GRAZING OCCULTATIONS

Prepared by Graham Blow

GRAZE OF ZC 3106 -1984 MARCH 27

Masterton, New Zealand le Librations

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PLANETARY OCCULTATIONS DURING 1984-5

[The remainder of this issue is a continuation ofthe article "Planetary Occultations During 1984," byDavid Dunham, which began in o.n. 3 (6), pp. 119-

146, and was continued in o.n. 3 (7), pp. 151-156,and in o.n. 3 (8), pp. 170-178. World maps are byMitsuru SOma. Regional maps and finder charts areby David Dunham.]

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